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We performed detailed chemical abundance analysis of the extremely metal-poor([Ar/H]-2) halo planetary nebula H4-1 based on the multi-wavelength spectrafrom Subaru/HDS, GALEX, SDSS, and Spitzer/IRS and determined the abundances of10 elements. The C and O abundances were derived from collisionally excitedlines (CELs) and are almost consistent with abundances from recombination lines(RLs). We demonstrated that the large discrepancy in the C abundance betweenCEL and RL in H4-1 can be solved using the temperature fluctuation model. Wereported the first detection of the [Xe III]5846 A line in H4-1 anddetermination of its elemental abundance ([Xe/H]>+0.48). H4-1 is the mostXe-rich PN among the Xe-detected PNe. The observed abundances are close to thetheoretical prediction by a ~2.0 Msun single star model with initiallyr-process element rich ([r/Fe]=+2.0 dex). The observed Xe abundance would be aproduct of the r-process in primordial SNe. The [C/O]-[Ba/(Eu or Xe)] diagramsuggests that the progenitor of H4-1 shares the evolution with two types ofcarbon-enhanced metal-poor stars (CEMP), CEMP-r/s and CEMP-no stars. Theprogenitor of H4-1 is a presumably binary formed in an r-process richenvironment.

Chemical abundances in the extremely Carbon and Xenon-rich halo planetary nebula H4-1